Transcript Application of AdS/CFT Correspondence to Non

Application of AdS/CFT
Correspondence to
Non-equilibrium Physics
Shin Nakamura
(Chuo University)
中央大学理工学部
Hadron physics ≈ Many-body physics
A possible direction to extend our research activity
is to challenge fundamental problems in many-body
physics that are common to wide range of physics,
not only in QCD but also in condensed matter physics.
My challenge here:
Non-equilibrium physics
Non-equilibrium Physics
Difficulty in non-equilibrium physics:
There is no powerful guiding principle
to predict the distribution.
• For equilibrium classical systems:
Maximization of entropy leads us to
the Maxwell-Boltzmann distribution.
• For equilibrium quantum systems:
The principle of detailed balance leads us to
the Bose/Fermi distributions.
Do we always need
these guiding principles?
No.
Some differential equation knows what
the thermal distribution is.
Einstein’s equation
The black hole solution has the notions of
• temperature
• entropy
• free energy
but of what?
AdS/CFT correspondence
[J. Maldacena, 1997]
The AdS/CFT correspondence answers to the question:
Some class of
black-hole geometries
AdS/CFT
Finite-temperature
states of gauge theories
[E. Witten, 1998]
The corresponding microscopic theory has been identified
through the AdS/CFT correspondence.
E.g.
AdS-Schwarzschild black hole in 5d
N=4 Super-Yang-Mills in 4d
at finite temperature
How much does the gravity dual know
the non-equilibrium physics?
Realization of
non-equilibrium states
1. We start with thermal equilibrium.
We can prepare the thermal equilibrium states
by using black hole geometry.
2. Then, we introduce an external force to drive
the system into non-equilibrium.
The black-hole solution will be deformed into
another solution which satisfies the boundary
condition corresponding to the external force.
Realization of
non-equilibrium states
If we follow this idea, all we need to do
in the gravity dual is to solve the equations
of motion under the boundary conditions
which take care of the external force.
This sounds feasible.
A good place to attack:
Non-equilibrium Steady State
Classification of Non-equilibrium States
Time independent
Linear-response regime
(Near equilibrium)
Out of the
linear-response regime
(Far from equilibrium)
Time dependent
Linear-response theory, hydrodynamics,......
We attack here.
Non-equilibrium Steady States (NESS)
Non-equilibrium steady state (NESS)
Non-equilibrium, but time-independent.
A typical example:
A system with a constant current along the electric field.
E
Air
J
• It is non-equilibrium, because heat and entropy are produced.
• The macroscopic variables can be time independent.
In order to realize a NESS, we need
an external force and a heat bath.
Setup for NESS
External force and heat bath are necessary.
Power supply drives the system our of equilibrium.
In large-Nc gauge theories:
Flow of energy
Work
External force
(E.g. Electric field)
We want to make
this NESS
“External force acting
on the quark charge”
“Flavor sector”
(“Quark sector”)
The system in study
Dissipation
dissipation
Heat bath
“Gluon sector”
(E.g. Air)
The subsystem can be NESS if the work of the source and the
energy dissipated into the heat bath are in balance.
Correspondence
A strongly-interacting
quantum gauge theory
Heat bath
(gluons)
Charged particle(s)
(quarks)
in the heat bath
AdS/CFT
equivalent
A classical gravity
(general relativity)
on a curved spacetime
in higher dimensions.
Black Hole
Object immersed
in the black hole
geometry
D-brane
D-brane
• A solitonic object in superstring theory.
It is like a membrane-like object.
(Dp-brane: (p+1)-dimensional object)
• A gauge theory can live on it.
D-brane
Gauge theory
Non-equilibrium steady states
in AdS/CFT
Thermal
equilibrium
strong external force
time evolution
Non-equilibrium state,
far from equilibrium
Classical theory
Black hole
gluons: heat bath
D-brane
quarks: charged particles
external force
acting on
the D-brane
Black hole
Still the same heat bath
D-brane
Driven to NESS
The classical mechanics of D-brane with electric
field in the black hole geometry tells the physics of NESS.
My related works
Physics in non-equilibrium steady states (NESS)
• Non-equilibrium phase transitions
S.N. Prog. Theor. Phys. 124 (2010) 1105.
S.N. Phys. Rev. Lett. 109 (2012) 120602.
• Effective temperature in NESS
S.N. and H. Ooguri, PRD88 (2013) 126003.
Cartoon
[Karch and O’Bannon, 2007]
E
D-brane
boundary
r
horizon

U(1) gauge field
on the D-brane
LDBI  e   det  a X   b X  g   Fab

We apply an external electric field E.
A1   Et  h(r )
J
L
Fr1
Relationship between E and J
[Karch and O’Bannon, 2007]
Fr1 
2
2
E
 g tt g xx
g
2
rr
J
g tt J 2  e  2 g tt g xxq 1
q: number of spatial directions
of the dual field theory.
Again, we have a special point r* given by
E 2  g tt g xx  0,
and J is given by
J 2  e 2 g tt g xxq 1
r*
0
in terms of E.
Cartoon
[Karch and O’Bannon, 2007]
E
D-brane
boundary
horizon
r
L
J
Fr1
We have a special point r=r* .
This plays a role of “horizon” for
the fluctuations of the electro-magnetic
field on the D-brane.
(See also [Gubser 2008, Kim-Shock-Tarrio 2011, Sonner-Green 2012])
Effective horizon
The effective horizon appears at r=r*.
E
D-brane
boundary
r
horizon
Small fluctuation of electro-magnetic field on D-brane δAb obeys to
the Maxwell equation on a curved geometry:
a


 g g ab  f bc g cd  0,
 f bc   bAa   aAb .
The metric is proportional to the open-string
metric, but is different from the induced metric.
The geometry has a horizon at r=r*.
(See also [Kim-Shock-Tarrio 2011, Sonner-Green 2012])
Now we have two temperatures
r=rH
r=r*
Black hole horizon
gives the temperature
of the heat bath.
r
boundary
The effective horizon on the string
gives a different “Hawking temperature”
that governs the fluctuations of the
test particle.
We call this effective temperature Teff of NESS.
If the system is driven to NESS,
rH<r* at the order of E2.
Two temperatures appear only in the non-linear regime.
Computations of
effective temperature
[S. N. and H. Ooguri, PRD88 (2013) 126003]
We have computed Teff for wide range of models.
• Heat bath:
Near-horizon geometry of Dp-brane solution at T.
[Itzhaki-Maldacena-Sonnenschein-Yankielowitcz, 1998]
ds  r
2
7 p
2
 1 
r07 p
r 7 p


dr 2
2
2
dt  dx 
r
7 p
2
1 
r07 p
r 7 p

p 3
2
 r d82 p
• Test particle: probe D(q+1+n)-brane or F1 string
wrapped on n-sphere
• Charged particles: probe D(q+1+n)-brane
Behavior of effective temperature
Beyond the linear
response regime
Teff  c01
c T 
c T 
142 p
5 p
0
142 p
5 p
0

E 
 CE
2
2
1/ 2
1
7 p
1
2  E2
4

 T   C 
T

O
(
E
)
142 p
2
7  p  c0T  5 p
1
p 3 
c0  74p , C   q  3  p 
n 
2
7 p 
This can be negative.
E.g. : D4-D2 system (p=4, q=2, n=0)
Teff < T can happen.
The temperature seen by fluctuations can be made
smaller by driving the system into NESS in some cases.
Is Teff<T allowed?
It is not forbidden.
Some examples of smaller effective temperature:
[K. Sasaki and S. Amari, J. Phys. Soc. Jpn. 74, 2226 (2005)]
[Also, private communication with S. Sasa]
Is it OK with the second law?
No contradiction.
• NESS is an open system.
• The second law of thermodynamics applies to
a closed system.
• The definition of entropy in NESS (beyond the
linear response regime) is not clear.
What is the physical meaning of Teff?
Fluctuation of electro-magnetic
fields on the D-brane
Fluctuation of current density
Computations of correlation functions of fluctuations in the gravity dual
is governed by the ingoing-wave boundary condition at the effective horizon.
 dt  f (t ) f (0)
v0
Im G R ( )
 2Teff
 0 ,

v0
fluctuation
dissipation
See also, [Gursoy et al.,2010]
The fluctuation-dissipation relation at NESS is characterized by
the effective temperature (at least for our systems).
Thermodynamics in NESS?
??
dE  Teff dS
It is highly nontrivial.
Hawking radiation (Hawking temperature) is more
general than the thermodynamics of black hole.
Hawking radiation:
It occurs as far as the “Klein-Gordon equation” of fluctuation
has the same form as that in the black hole.
Thermodynamics of black hole:
We need the Einstein’s equation. It relies on the theory of gravity.
Example of “non-gravity”
Hawking radiation
Sonic black hole in liquid helium.
Fast
Sonic horizon where the flow velocity
exceeds the velocity of sound.
Slow
• The sound cannot escape from inside the “horizon”.
• It is expected that the sonic horizon radiates a “Hawking
radiation” of sound at the “Hawking temperature”.
[W. G. Unrhu, PRL51(1981)1351]
However, any “thermodynamics” associated with the
Hawking temperature of sound has not been established so far.
[See for example, M. Visser, gr-qc/9712016 ]
Summary
At least for some examples of NESS:
• There exists two temperatures in the non-linear regime.
• The effective temperature appears in terms of the
Hawking temperature at the effective horizon.
• It agrees with the coefficient in the generalized
fluctuation-dissipation relation in NESS.
• Teff < T can occur for some cases.
Hint for non-equilibrium physics from AdS/CFT
Acknowledgement
• I was a member of “New Hadron Project”
as a postdoc for 3 years at Kyoto University.
• I was also working for 1 year here in Nagoya.
Without these experience in the community
of quark-hadron physics, I would have never
reached my current research and my current
position.
Backup slides
Nontrivial problems of SSB
(Jona-Lasinio, 2010)
SSB in non-equilibrium processes
Superfluid He flow : Bose condensation
of NG phonon modes
1-D phase transition not possible, but
1-D highway traffic model (Popkov et al 2008)
>------------ ↘ _________ ↗ ------------->
<------------ ↗
↘ -------------<
Role of SSB in cosmology?
Prof. Y. Nambu’s slide @ Baryons’10
What is temperature?
Definitions of effective temperature:
Pe
ET
1
t

t

, E E T
dE  TdS
f
eff v
Thermodynamics
D T
diffusion const.
differential mobility
Fluctuation-dissipation
relation
They give the same temperature.
 a 
a
b
Killing vector
Eff. Horizon
Distributions
 2Teff 
Hawking
b
temperature
Eff. Horizon
What is temperature?
Definitions of effective temperature:
Pe
E
Teff
1
t

t

, E E T
dE  TdS
f
eff v
Thermodynamics
D T
diffusion const.
differential mobility
Fluctuation-dissipation
relation
They give the same temperature.
 a 
a
b
Killing vector
Eff. Horizon
Distributions of
small fluctuations
 2Teff 
Hawking
b
temperature
Eff. Horizon